Catalogs of Compact Groups of Galaxies From the Enhanced SDSS Dr12

Sohn, Jubee; Geller, Margaret J.; Hwang, Ho Seong; Zahid, H. Jabran; Lee, Myung Gyoon

doi:10.3847/0067-0049/225/2/23

Cited by 29 publications

(70 citation statements)

References 90 publications

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“…This methodology has been used to construct similar catalogues using surveys such as the COSMOS-UKST Southern Galaxy Catalogue (Iovino 2002), 2MASS (Díaz-Giménez et al 2012Zandivarez 2015), andSDSS (McConnachie et al 2009). Compact groups have also been identified using the FoF algorithm on surveys such as the CfA2 (Barton et al 1996), and SDSS (Sohn et al 2016); however, incompleteness due to fibre collsions particularly disrupts dense, compact structures, such as compact groups. Recent work has advocated for combining the two selection methods, for example, Díaz-Giménez et al (2018) using SDSS, and Zheng & Shen (2020) who combined redshift information from SDSS, LAMOST, and GAMA.…”

Section: Compactnessmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA): Demonstrating the Power of WISE in the Study of Galaxy Groups to z < 0.1

Cluver

Jarrett

Taylor

et al. 2020

ApJ

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Combining high-fidelity group characterisation from the Galaxy and Mass Assembly (GAMA) survey and source-tailored z < 0.1 photometry from the WISE survey, we present a comprehensive study of the properties of ungrouped galaxies, compared to 497 galaxy groups (4≤ N FoF ≤ 20) as a function of stellar and halo mass. Ungrouped galaxies are largely unimodal in WISE color, the result of being dominated by star-forming, late-type galaxies. Grouped galaxies, however, show a clear bimodality in WISE color, which correlates strongly with stellar mass and morphology. We find evidence for an increasing earlytype fraction, in stellar mass bins between 10 10 M stellar 10 11 M , with increasing halo mass. Using ungrouped, late-type galaxies with star-forming colors (W2−W3>3), we define a star-forming mainsequence (SFMS), which we use to delineate systems that have moved below the sequence ("quenched" for the purposes of this work). We find that with increasing halo mass, the relative number of latetype systems on the SFMS decreases, with a corresponding increase in early-type, quenched systems at high stellar mass (M stellar > 10 10.5 M ), consistent with mass quenching. Group galaxies with masses M stellar < 10 10.5 M show evidence of quenching consistent with environmentally-driven processes. The stellar mass distribution of late-type, quenched galaxies suggests they may be an intermediate population as systems transition from being star-forming and late-type to the "red sequence". Finally, we use the projected area of groups on the sky to extract groups that are (relatively) compact for their halo mass. Although these show a marginal increase in their proportion of high mass and early-type galaxies compared to nominal groups, a clear increase in quenched fraction is not evident.

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Section: Compactnessmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA): Demonstrating the Power of WISE in the Study of Galaxy Groups to z < 0.1

Cluver

Jarrett

Taylor

et al. 2020

ApJ

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“…The FoF algorithm have been used to build galaxy group catalogues for most major astronomical surveys, including Sloan Digital Sky Survey (Merchán & Zandivarez 2005;Berlind et al 2006;Deng et al 2007;Tago et al 2008Tago et al , 2010Muñoz-Cuartas & Müller 2012;Tempel et al 2012Tempel et al , 2014bTempel et al , 2017Sohn et al 2016), GAMA (Robotham et al 2011), Millennium Galaxy and Group Catalogue (Calvi et al 2011), and 2dF galaxy redshift survey (Merchán & Zandivarez 2002;Eke et al 2004;Tago et al 2006). FoF algorithm has a long history in astronomy and it is actively used since Turner & Gott (1976).…”

Section: Introductionmentioning

confidence: 99%

Bayesian group finder based on marked point processes

Tempel

Kruuse

Kipper

et al. 2018

A&A

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Context. Galaxy groups and clusters are formidable cosmological probes. They permit the studying of the environmental effects on galaxy formation. A reliable detection of galaxy groups is an open problem and is important for ongoing and future cosmological surveys. Aims. We propose a probabilistic galaxy group detection algorithm based on marked point processes with interactions. Methods. The pattern of galaxy groups in a catalogue is seen as a random set of interacting objects. The positions and the interactions of these objects are governed by a probability density. The parameters of the probability density were chosen using a priori knowledge. The estimator of the unknown cluster pattern is given by the configuration of objects maximising the proposed probability density. Adopting the Bayesian framework, the proposed probability density is maximised using a simulated annealing (SA) algorithm. At fixed temperature, the SA algorithm is a Monte Carlo sampler of the probability density. Hence, the method provides “for free” additional information such as the probabilities that a point or two points in the observation domain belong to the cluster pattern, respectively. These supplementary tools allow the construction of tests and techniques to validate and to refine the detection result. Results. To test the feasibility of the proposed methodology, we applied it to the well-studied 2MRS data set. Compared to previously published Friends-of-Friends (FoF) group finders, the proposed Bayesian group finder gives overall similar results. However for specific applications, like the reconstruction of the local Universe, the details of the grouping algorithms are important. Conclusions. The proposed Bayesian group finder is tested on a galaxy redshift survey, but more detailed analyses are needed to understand the actual capabilities of the algorithm regarding upcoming cosmological surveys. The presented mathematical framework permits adapting it easily for other data sets (in astronomy and in other fields of sciences). In cosmology, one promising application is the detection of galaxy groups in photometric galaxy redshift surveys, while taking into account the full photometric redshift posteriors.

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“…In addition to the limitations in volume, if the projected distance between individual members is very small (as typical for CGs) both observations and simulations are prone to missing group members in different ways. While redshift dependent fiber collision and blending (see discussions in Mamon 2010 andSohn et al 2016) can occur in observations, the exact identification of close pair members (major mergers) depends on the substructure finder used in 3 The halo mass M 200,crit is defined as the mass that encloses a mean density of 200 times the critical density of the Universe. simulations (e.g.…”

Section: Discussionmentioning

confidence: 99%

Abundance and group coalescence time-scales of compact groups of galaxies in the EAGLE simulation

Hartsuiker

Ploeckinger

2019

Monthly Notices of the Royal Astronomical Society: Letters

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Observations of compact groups of galaxies (CGs) indicate that their abundance has not significantly changed since z = 0.2. This balance between the timescales for formation and destruction of CGs is challenging if the typical timescale for CG members to merge into one massive galaxy is as short as historically assumed (< 0.1 Hubble times). Following the evolution of CGs over time in a cosmological simulation (EA-GLE), we quantify the contributions of individual processes that in the end explain the observed abundance of CGs. We find that despite the usually applied maximum line-of-sight velocity difference of 1000 km s −1 within the group members, the majority of CGs (≈ 60 per cent) are elongated along the line-of-sight by at least a factor of two. These CGs are mostly transient as they are only compact in projection. In more spherical systems ≈ 80 per cent of galaxies at z > 0.4 merge into one massive galaxy before the simulation end (z = 0) and we find that the typical timescale for this process is 2-3 Gyr. We conclude that the combination of large fractions of interlopers and the longer median group coalescence timescale of CGs alleviates the need for a fast formation process to explain the observed abundance of CGs for z < 0.2.

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Catalogs of Compact Groups of Galaxies From the Enhanced SDSS Dr12

Cited by 29 publications

References 90 publications

Galaxy and Mass Assembly (GAMA): Demonstrating the Power of WISE in the Study of Galaxy Groups to z < 0.1

Galaxy and Mass Assembly (GAMA): Demonstrating the Power of WISE in the Study of Galaxy Groups to z < 0.1

Bayesian group finder based on marked point processes

Abundance and group coalescence time-scales of compact groups of galaxies in the EAGLE simulation

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